The rise of the Milky Way disk through EMP stars
We present a chemo-dynamical study conducted with 2dF+AAOmega of ∼ 6 000 Gaia DR3 non-variable candidate metal-poor stars that lie in the direction of the Galactic plane. Our spectral analysis reveals 15 new extremely metal-poor (EMP) stars, with the lowest metallicity at [Fe/H] = −4.0 ± 0.2 dex. Tw...
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| Main Authors: | , , , , , , , , |
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| Format: | Article (Journal) |
| Language: | English |
| Published: |
20 March 2025
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| In: |
Publications of the Astronomical Society of Australia
Year: 2025, Volume: 42, Pages: 1-23 |
| ISSN: | 1448-6083 |
| DOI: | 10.1017/pasa.2025.16 |
| Online Access: | Verlag, kostenfrei, Volltext: https://doi.org/10.1017/pasa.2025.16 Verlag, kostenfrei, Volltext: https://www.cambridge.org/core/journals/publications-of-the-astronomical-society-of-australia/article/rise-of-the-milky-way-disk-through-emp-stars/EFF26A5C409854F3FADFE9BD19306359 
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| Author Notes: | Benjamin David Caleb Lowe, Thomas Nordlander, Luca Casagrande, Gary S. Da Costa, Michael Bessell, Madeleine McKenzie, Giacomo Cordoni, Norbert Christlieb, and Sven Buder |
| Summary: | We present a chemo-dynamical study conducted with 2dF+AAOmega of ∼ 6 000 Gaia DR3 non-variable candidate metal-poor stars that lie in the direction of the Galactic plane. Our spectral analysis reveals 15 new extremely metal-poor (EMP) stars, with the lowest metallicity at [Fe/H] = −4.0 ± 0.2 dex. Two of the EMP stars are also carbon enhanced, with the largest enhancement of [C/Fe] = 1.3 ± 0.1 occurring in a dwarf. Using our [C/Fe] results, we demonstrate that the number of carbon-depleted stars decreases with lower metallicities, and the fraction of carbon-enhanced stars increases, in agreement with previous studies. Our dynamical analysis reveals that the fraction of prograde and retrograde disk stars, defined as zmax < 3 kpc, with Jφ /Jtot > 0.75 and Jφ /Jtot < −0.75, respectively, changes as metallicities decrease. Disk stars on retrograde orbits make up ∼ 10% of all the stars in our sample with metallicities below −2.1 dex. Interestingly, the portion of retrograde disk stars compared with the number of kinematically classified halo stars is approximately constant at 4.6% for all metallicities below −1.5 dex. We also see that Jφ increases from 380 ± 50 to 1320 ± 90 km s−1 kpc across metallicity range −1.5 to −1.1, consistent with the spin-up of the Galactic disk. Over the metallicity range −3.0 < [Fe/H] < −2.0, the slopes of the metallicity distribution functions for the prograde and retrograde disk stars are similar and comparable to that for the halo population. However, detailed chemical analyses based on high-resolution spectra are needed to distinguish the accreted versus in situ contributions. Finally, we show that our spectroscopic parameters reveal serious systematics in the metallicities published in recent studies that apply various machine learning techniques to Gaia XP spectra. |
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| Item Description: | Gesehen am 03.11.2025 |
| Physical Description: | Online Resource |
| ISSN: | 1448-6083 |
| DOI: | 10.1017/pasa.2025.16 |